Abstract
The triangular Lagrangian points of the elliptic restricted three-body problem (ERTBP) with oblate and radiating more massive primary are studied. The mean motion equation used here is different from the ones employed in many studies on the perturbed ERTBP. The effect of oblateness on the mean motion equation varies. This change influences the location and stability of the triangular Lagrangian points. The points tend to shift in the y-direction. The influence of the oblateness on the critical mass ratio is also altered. But the eccentricity limit  for stability remains the same.  Â
Highlights
Because of their stable location and many other advantages particular to the chosen system and the positions, the Lagrangian points are of practical interests from the late 20th century [2]
The points became system-specific with the inclusion of perturbations [7 - 10]. These perturbations directly affected the equations of motion and the mean motion equation, which in turn influenced the properties of the Lagrangian points
The rectified mean motion equation is used here. This mean motion equation is obtained from the secular perturbation effects of oblateness [12]
Summary
Because of their stable location (due to nullified centrifugal and gravitational forces [1]) and many other advantages particular to the chosen system and the positions, the Lagrangian points are of practical interests from the late 20th century [2]. They serve to be the address for many natural (Trojan asteroids) and artificial satellites. This paper intends to employ the newly formulated mean motion equation [11] to the elliptic restricted three-body problem (ERTBP) considering the more massive primary as an oblate and radiating spheroid and the other primary as a point mass. The transition curves are generated to collectively show the region of stability in the eccentricity – mass ratio plane
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